where \(L\)  is the characteristic scale of the density structure in cold interstellar phases
[1]}, [2]}
and \(V_L\)  is of the order of shock velocity,
[3]}
found that the turbulent dynamo in the shock precursor is entirely in the damping stage as shown in
Fig. REF .
Here \(n_H\)  and \(n_e\)  are number densities of the atomic hydrogen and electrons, and \(T\)  is the temperature
[4]}.
The timescale of the dynamo \(\tau _\text{dam}\) ,
\(\tau _\text{dam} = \frac{23}{3} \Big (\frac{L}{V_L} - \Gamma _\nu ^{-1} \Big ) ,\) 
